Catalog of Solar Particle Events 1955–1969: Prepared under the Auspices of Working Group 2 of the Inter-Union Commission on Solar-Terrestrial Physics

432 Pages·1975·20.22 MB·English

by  H. W. Dodson, E. R. Hedeman, R. W. Kreplin, M. J. Martres, V. N. Obridko, M. A. Shea, D. F. Smart, H. Tanaka (auth.), Z. à vestka, P. Simon (eds.)

CATALOG OF SOLAR PARTICLE EVENTS
1955-1969
ASTROPHYSICS AND
SPACE SCIENCE LIBRARY
A SERIES OF BOOKS ON THE RECENT DEVELOPMENTS
OF SPACE SCIENCE AND OF GENERAL GEOPHYSICS AND ASTROPHYSICS
PUBLISHED IN CONNECTION WITH THE JOURNAL
SPACE SCIENCE REVIEWS
Editorial Board
J. E. BLAMONT, Laboratoire d'Aeronomie, Verrieres, France
R. L. F. BOYD, University College, London, England
L. GOLDBERG, Kitt Peak National Observatory, Tuscon, Ariz., U.S.A.
I
C. DE JAGER, University of Utrecht, Holland
Z. KOPAL, University of Manchester, Manchester, England
G. H. LUDWIG, NOAA, National Environmental Satellite Service, Suitland, Md., U.S.A.
R. LUST, Institutfiir Extraterrestrische Physik, Garching-Mjjnchen, Germany
B. M. MCCORMAC, Lockheed Palo Alto Rese~rch Laboratory, Palo Alto, Calif., U.S.A.
H. E. NEWELL, NASA, Washington, D.C., U.S.A.
L. I. SEDOY, Academy of Science of the U.S.S.R., Moscow, U.S.S.R.
Z. SYESTKA, American Science and Engineering, Cambridge, Mass., U.S.A.
Secretary of the Editorial Board
w. DE GRAAFF, Sterrewacht 'Sonnenborgh', University of Utrecht, Utrecht, Holland
VOLUME 49
CATALOG
OF SOLAR PARTICLE EVENTS
1955-1969
Prepared under the Auspices of Working Group 2 of the Inter~Union Commission
on Solar-Terrestrial Physics by
H. W. DODSON and E. R. HEDEMAN
The McMath-Hulbert Observatory of the University of Michigan, Pontiac, Mich., U.S.A.,
R. W. KREPLIN
The Naval Research Labaratory, Washington, D.C., U.S.A.,
M. J. MAR TRES
Observatoire de Paris, Meudon. France
V. N. OBRIDKO
IZMIRAN Moscow. U.S.S.R.
M. A. SHEA and D. F. SMART
Air Force Cambridge Research Labaratories, Bedford, Mass., U.S.A.
H. TANAKA
Research Institute of Atmospherics, Toyokawa, Japan
edited by
Z. SVESTKA
Fraunhofer Institute, Freiburg im Breisgau, F.R.G.,
presently at American Science and Engineering, Cambridge, Mass., U.S.A.
P. SIMON
Observatoire de Paris, Meudon, France
with the assistance of L. FRITZOvA-8VESTKovA (Freiburg and Cambridge) and A. GUITART (Meudon)
D. REIDEL PUBLISHING COMPANY
DORDRECHT-HOLLAND / BOSTON-U.S.A.
Library of Congress Catalog Card Number 74-81944
ISBN-13: 978-94-010-1744-2 e-ISBN-13: 978-94-010-1742-8
DOl: 10.1007/978-94-010-1742-8
Published by D. Reidel Publishing Company
P.O. Box 17, Dordrecht, Holland
Sold and distributed in the U.S.A., Canada, and Mexico
by D. Reidel Publishing Company, Inc.
306 Dartmouth Street, Boston,
Mass. 02116, U.S.A.
All Rights Reserved
Copyright © 1975 by D. Reidel Publishing Company, Dordrecht, Holland
Softcover reprint of the hardcover 1st edition 1975
No part of this book may be reproduced in any form, by print, photoprint, microfilm,
or any other means, without written permission from the publisher
TABLE OF CONTENTS
PREFACE VII
ACKNOWLEDGEMENTS IX
INTRODUCTION
Part 1
Appendix A 7
Part 2 8
Part 3 10
Appendix B 11
27-day Index 12
Appendix 1 to the Introduction - Electron Contamination 12
Appendix 2 to the Introduction - Criteria for the Association of Solar
Phenomena with the Particle Events 18
Appendix 3 to the Introduction - Sensitivity Levels of the Various Detectors 19
PART 1
Catalog of Solar Particle Events, 1955-1969 25
A P PEN D I X A - List of Unconfirmed and Low-Energy Proton Events and of Pure
Electron Events, Omitted in Part 1 119
PART 2
List of Flares which have been Identified as Sources of Particle Events 143
References to Parts 1 and 2 and Appendix A 237
PART 3
Maps of Selected Active Regions which were Sources of Particle Events 243
A P PEN D I X B - List of Active Regions which were Sources of Particle Events 373
References to Part 3 and Appendix B 401
27-day Index of Solar Particle Events, 1955-1969 411
PREFACE
This Catalog originated as a common enterprise of solar physicists and space scientists
under the auspices of the Second Working Group of the Inter-Union Commission of Solar
Terrestrial Physics (IUCSTP). It is a pleasure to acknowledge the support we received
from the IUCSTP president, Dr H. Friedman, and the IUCSTPSecretary, Dr E. R. Dyer
during the several years we have spent on this project.
The aim of our work has been to assemble all observations of particle events from the
first PCA observation in 1955 through two solar cycle maxima up to the end of 1969, in
order to preserve these data from the first epoch of the space era in a concise form for use
in the future. Because the techniques of observation have very much improved in the present
solar cycle, there is a tendency to consider the observations before 1964 as incomplete
and out-of-date; one must not forget, however, that the 19th solar cycle greatly differed
from cycle No. 20 in the level of its activity, and also may have been the last cycle of strong
activity for many decades to come. Therefore, the particle event observations before 1964
'should be compiled in a consistent manner for comparison with later observations, and
we believe that the Catalog achieves this.
The rapid development of the exploration techniques necessarily results in a significant
amount of inhomogeneity in the Catalog, as increasingly smaller events were detected.
This lack of homogeneity cannot be avoided and the reader should be well aware of its
existence. Before using the Catalog, a careful reading of the Introduction is essential.
The Catalog consists of three Parts. For Part 1 and Appendix A, M. A. Shea and
D. F. Smart have summarized observations of particle increases during the 15 years stud-
ied. In addition to the excerption of published data many unpublished observations were
included through the cooperation of K. A. Anderson, R. P. Bukata, J. R. Burrows, C. Y. Fan,
M. Gros, M. van Hollebeke, S. W. Kahler, H. Leinbach, R. P. Un, K. G. McCraken,
F. B. McDonald, A. J. Masley, U. R. Rao, J. A. Simpson, S. Singer, S. N. Vernov, and
J. R. Wang, to all of whom our particular thanks are due. A significant contribution to
the list of ground-based data was made by E. R. Hedeman, and the list of PCA events prior
to 1964 was checked by G. C: Reid.
In a very detailed and careful study H. W. Dodson and E. R. Hedeman have tried to find
the source, or alternative sources, of each particle event in Part 1 of the Catalog, or in
Appendix A, using criteria explained in the Introduction. Their work has clearly demon-
strated how difficult it is to find the actual sources of the particles on the Sun, as soon as
the study is extended to particle events of relatively low energy.
The final selection of the events to be included in Part 1 of the Catalog or Appendix A,
respectively, the choice of abbreviated selected data to be published on each event, and
the final association with solar and interplanetary sources, has been made by the Editors
(by Svestka for 1955-1966, and by Simon for 1967-1969). The opinions ofH. Tanaka
(radio emission) and R. W. Kreplin (X-ray bursts) were a helpful tool when checking the
associations suggested by H. W. Dodson and E. R. Hedeman.
VIII PREFACE
All the flares which have been considered to be obvious or probable sources of particle
events are listed in Part 2, with a brief description of their characteristic features. This
part was prepared by the Editors (for the same periods as above), using a summary of radio
events prepared by H. Tanaka, and a list of X-ray bursts prepared by R. W. Kreplin.
Unpublished X-ray data have been made available by J. P. Conner, S. R. Kane, S. Singer,
and Ch. Wende. Extensive use has been made of data published in the Quarterly Bulletin
on Solar Activity (Zurich) and the Solar-Geophysical Data (Boulder). The final arrange-
ment of Parts 1 and 2 was made by L. Fritzova-Svestkova and A. Guitart.
Finally, Part 3 contains a description of the active regions on the Sun, in which the
flares of Part 2 occurred. M. J. Martres has prepared the basic section of this part, having
received considerable support from many solar observatories: Athens (Greece), Boulder
and Carnarvon (WDC-A Boulder, U.s.A.), Culgoora (CSIRO, Australia), Debrecen
(Hungary), Capri F (Fraunhofer Institute, Freiburg, F.R.G.), Honolulu and Haleakala
(Hawaii, U.S.A.), Lockheed (U.S.A.), McMath-Hulbert (pontiac, U.S.A.), Meudon and St.
Michel de Haute Provence (France), Mitaka (Japan), Mt. Wilson (U.S.A.), Capri S (Salts-
jobaden, Sweden), Tashkent and Voroshilov (U.S.S.R.). Appendix B and the references
to Part 3 were prepared by V. N. Obridko, with the assistance of Y. N. Dolginova and
E. V. Ivanov. Since this section differed in some aspects from the style of the other parts
of the Catalog, it has been rearranged, renumbered, and transliterated by the Meudon
librarian, M. Guidoni. Nevertheless, this Appendix remains a somewhat less homogeneous
constituent of the Catalog, since the latest changes and improvements of Part 1 could not
be reflected fast enough.in Obridko's laborious system of references.
Finally I must say that I greatly underestimated the extent of this work when I first
proposed it in 1969. Therefore, I deeply admire all the authors and my co-editor, since
they never hesitated to continue, even when the work continuously expanded. Let me
express my deep gratitude to all of them for their enthusiastic approach to the enormous
amount of work we had to do. P. Simon's and my particular thanks are extended to
M. A. Shea and D. F. Smart of Bedford, H. W. Dodson and E. R. Hedeman of Pontiac,
and M. J. Martres of Meudon, who carried the main burden of this enterprise.
Freiburg, 31 December, 1973 ZDENEK SVESTKA
Chairman
IUCSTP Working Group 2
ACKNOWLEDGEMENTS
This Catalog could not have been accomplished without the assistance of many scientists
throughout the world. Our particular thanks are extended to:
J. A. SIMPSON for unpublished data from IMP 1,2,3, and 4;
J. A. SIMPSON and C. Y. FAN for unpublished data from Pioneers 6 and 7;
S. N. VERNOV for a special list of the U.S.s.R. observations of proton increases in the
stratosphere and interplanetary space;
K. A. ANDERSON and R. P. LIN for unpublished data on solar electron events;
J. H. KING and the U.s. National Space Science Data Center for their cooperation in
providing considerable satellite data;
L. DESZO for white-light solar photographs specially prepared for the Catalog by the staff
of the Debrecen Observatory;
J. RAY ROLE and 1. SORU ESCAUT for the magnetic field data from Meudon;
We also express our gratitude to
G. C. REID for checking the list of the PCA events;
M. VAN HOLLEBEKE, J. R. WANG, and F. B. McDONALD for unpublished data from
IMP 4;
S. KAHLER, S. R. KANE, and K. A. ANDERSON for unpublished OGO data;
K. G. McCRACKEN, U. R. RAO, and R. P. BUKATA for unpublished data from Pioneers
6 and 7;
J. R. BURROWS for unpublished Alouette I data;
J. P. CONNER for unpublished X-ray data from the VELA 3A and 3B satellites;
M. GROS for unpublished HEOS data;
Ch. WENDE for unpublished X-ray data from Explorer 33;
S. SINGER for unpublished data from VELA 4; and
L. M. ADKINS, G. BANOS, A. BRUZEK, V. EVANS, G. HOSINSKY, J. V. LINCOLN,
M. McCABE, S. MARTIN, and F. MORYAMA for supplying optical and magnetic field
solar data.
Finally, we acknowledge with thanks private communications we received from
L. E. ANDERSON, J. R. ASBRIDGE, C. D. BOSTROM, F. B. McDONALD, K. C. HSIEH,
H. S. HUDSON, D. H. JELLY, A. J. MASLEY, H. LEINBACH, and D. J. WILLIAMS.
The aid we received from Y. N. DOLGINOVA and E. V. IVANOV in Moscow and
M. GUIDONI, J. GAPIHAN, and G. SERV AJEAN in Meudon when preparing the third
part of the Catalog is highly appreciated.
THE EDITORS
INTRODUCTION
Part 1
This part of the Catalog contains only confirmed particle events with> 10 MeV proton
flux in excess of 0.1 proton (cm2 s sterr' before December 1965, and in excess of 0.01
proton (cm2 s sterr' since December 1965. 'Confirmed' means that at least two indepen-
dent measurements indicate the existence of the event.
In the HEADING of each event we give its serial number, the date of the earliest onset
reported, an approximate onset time, and the importance of the event, according to the
classification system of Smart and Shea (1971), reproduced for reader's convenience in
Table I.
TABLE I
Solar proton event classification system (Smart and Shea, 1971)
First digit Second digit Third digit
Digit > 10 MeV proton Daylight polar Sea level
flux (cm' s sterfl cap absorption neutron monitor
at 30 MHz increase
-2 10-'-< 10-1
-1 10-1_< 10°
o 10°-<10 1 No increase No increase
1 10 1_<10' <1.5 dB <3%
2 10 2-< 10 3 1.5-<4.6 dB 3-<10%
3 10 3_< 10' 4.6-< 15 dB 10-< 100%
4 ;;. 10' ;;. 15dB ;;. 100%
x measurements not available
( ) the digit is uncertain or implied
Observed ground-based and/or space data on each particle event are arranged according
to the onset times below each heading. A complete line (all data is not always available)
comprises the following information:
FIRST COLUMN: Kind of observation or name of the spacecraft. The abbreviations used:
VHF very high frequency ionospheric scatter data for the polar cap absorptions
(Bailey, 1964);
[-min polar cap absorption measurements by means of ionosondes;
RIOM -30 MHz riometer measurements of polar cap absorptions;
[-fix polar cap absorption measurements by means of high-sensitivity backscatter
sounding of the lower ionosphere at 2.3 MHz (Gregory, 1963);
VLF polar cap absorption as measured from modifications of the propagation
of very low frequency waves;
2 INTRODUCTION
Pr>2.3 GeV neutron monitor record of an increase corresponding to the presence of
protons with energies in excess of2.3 GeV;
Balloon particle flux measurements carried out during a balloon flight;
Rocket particle flux measurements carried out during a rocket flight;
ALOU Alouette
EXPL Explorer
MAR Mariner
PION Pioneer
VEN Venus
SECOND COLUMN: Kind of particles and the energy range recorded. The abbreviations
used:
GLE ground level effect, implying> 500 MeV protons in the particle flux;
peA polar cap absorption, implying protons of the order of 10 MeV in the par-
ticle flux;
Pr>SS MeV specifies the energy range of protons. Most of the time, this is an abbrevi-
ation for an energy 'window' listed in Table II (for a given spacecraft and
reference). The absence of any information in Table II means that the
upper limit for the recorded energy is not specified by the experimenters.
El> 40 keV electrons with energies in excess of 40 ke V;
Pr 14 MeV differential flux measurement at the mean energy of the proton channel.
The lower edge of the channel is always given.
Pr (10-15 gr) protons penetrating to the balloon floating at altitudes corresponding to
10-15 grams of atmospheric depth.
THIRD COLUMN: Onset time of the particle event.
FOURTH COLUMN: Time of the maximum particle flux.
If not indicated otherwise, the time in these two columns refers to the day given in the
heading. Note that2Sh 10m = next day 01 h 10m.
Whenever the time refers to a day different from the date in the heading, the day is
added, e.g. 29d 14h2Sm.
In these two columns we also indicate the accuracy of the time given, according to the
following scheme:
the stations given in references give the time within these limits (the
earliest time being given in ref. (3));
22h40m ±02m an exact time between 22h38m and 42m ;
22hOOm the accuracy is not exactly known, but it is expected to be significantly
smaller than ± 30m;
the time accuracy is not known.
In all other cases we give a code:
Lll time accurate to within one hour;
Ll2 time uncertainty greater than one hour;
Ll3 start superimposed on enhancement of previous event;
Ll4 estimate because of magnetospheric perigee interference;
Ll5 missing data; or estimate because of missing data;
Ll6 estimate because of broad maximum;